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Science 4 July 1986:
Vol. 233. no. 4759, pp. 102 - 106
DOI: 10.1126/science.233.4759.102
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Articles

Voyager 2 Radio Observations of Uranus

JAMES W. WARWICK 1, DAVID R. EVANS 1, JOSEPH H. ROMIG 1, CONSTANCE B. SAWYER 1, MICHAEL D. DESCH 2, MICHAEL L. KAISER 2, JOSEPH K. ALEXANDER 3, THOMAS D. CARR 4, DAVID H. STAELIN 5, SAMUEL GULKIS 6, ROBERT L. POYNTER 6, MONIQUE AUBIER 7, ANDRE BOISCHOT 7, YOLANDE LEBLANC 7, ALAIN LECACHEUX 7, BENT M. PEDERSEN 7, and PHILIPPE ZARKA 7

1 Radiophysics, Inc., Boulder, CO 80301.
2 Laboratory for Extraterrestrial Physics, Goddard Space Flight Center, Greenbelt, MD 20771.
3 NASA Headquarters, Washington, DC, 20546.
4 Department of Astronomy, University of Florida, Gainesville, FL 32611.
5 Research Laboratory of Electronics, Massachusetts Institute of Technology, Cambridge, MA 02319.
6 Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109.
7 Observatoire de Paris, Section d'Astrophysique, 92190 Meudon, France.

Within distances to Uranus of about 6 x 106 kilometers (inbound) and 35 x 106 kilometers (outbound), the planetary radio astronomy experiment aboard Voyager 2 detected a wide variety of radio emissions. The emission was modulated in a period of 17.24 ± 0.01 hours, which is identified as the rotation period of Uranus' magnetic field. Of the two poles where the axis of the off-center magnetic dipole (measured by the magnetometer experiment aboard Voyager 2) meets the planetary surface, the one closer to dipole center is now located on the nightside of the planet. The radio emission generally had maximum power and bandwidth when this pole was tipped toward the spacecraft. When the spacecraft entered the nightside hemisphere, which contains the stronger surface magnetic pole, the bandwidth increased dramatically and thereafter remained large. Dynamically evolving radio events of various kinds embedded in these emissions suggest a Uranian magnetosphere rich in magnetohydrodynamic phenomena.

Submitted on March 28, 1986
Accepted on May 5, 1986


THIS ARTICLE HAS BEEN CITED BY OTHER ARTICLES:
Voyager Planetary Radio Astronomy at Neptune.
J. W. Warwick, D. R. Evans, G. R. Peltzer, R. G. Peltzer, J. H. Romig, C. B. Sawyer, A. C. Riddle, A. E. Schweitzer, M. D. Desch, M. L. Kaiser, et al. (1989)
Science 246, 1498-1501
   Abstract »    PDF »
Voyager 2 in the Uranian System: Imaging Science Results.
B. A. Smith, B. A. SMITH, L. A. SODERBLOM, R. BEEBE, D. BLISS, J. M. BOYCE, A. BRAHIC, G. A. BRIGGS, R. H. BROWN, S. A. COLLINS, et al. (1986)
Science 233, 43-64
   Abstract »    PDF »
Magnetic Fields at Uranus.
N. F. Ness, N. F. NESS, M. H. ACUNA, K. W. BEHANNON, L. F. BURLAGA, J. E. P. CONNERNEY, R. P. LEPPING, and F. M. NEUBAUER (1986)
Science 233, 85-89
   Abstract »    PDF »
Energetic Charged Particles in the Uranian Magnetosphere.
E. C. STONE, J. F. COOPER, A. C. CUMMINGS, F. B. MCDONALD, J. H. TRAINOR, N. LAL, R. MCGUIRE, and D. L. CHENETTE (1986)
Science 233, 93-97
   Abstract »    PDF »
The Magnetosphere of Uranus: Hot Plasma and Radiation Environment.
S. M. KRIMIGIS, T. P. ARMSTRONG, W. I. AXFORD, A. F. CHENG, G. GLOECKLER, D. C. HAMILTON, E. P. KEATH, L. J. LANZEROTTI, and B. H. MAUK (1986)
Science 233, 97-102
   Abstract »    PDF »
First Plasma Wave Observations at Uranus.
D. A. GURNETT, W. S. KURTH, F. L. SCARF, and R. L. POYNTER (1986)
Science 233, 106-109
   Abstract »    PDF »


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